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    Kozai Migration Naturally Explains the White Dwarf Planet WD1856 b

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    Author
    Muñoz, Diego J.
    Petrovich, Cristobal
    Affiliation
    Univ Arizona, Steward Observ
    Issue Date
    2020-11-19
    Keywords
    Binary stars
    White dwarf stars
    Exoplanet dynamics
    Exoplanet evolution
    Multiple stars
    
    Metadata
    Show full item record
    Publisher
    IOP PUBLISHING LTD
    Citation
    Muñoz, D. J., & Petrovich, C. (2020). Kozai Migration Naturally Explains the White Dwarf Planet WD1856 b. The Astrophysical Journal Letters, 904(1), L3.
    Journal
    ASTROPHYSICAL JOURNAL LETTERS
    Rights
    © 2020. The American Astronomical Society. All rights reserved.
    Collection Information
    This item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
    Abstract
    The Jovian-sized object WD.1856.b transits a white dwarf (WD) in a compact 1.4 day orbit. Unlikely to have endured stellar evolution in its current orbit, WD. 1856.b is thought to have migrated from much wider separations. Because the WD is old, and a member of a well-characterized hierarchical multiple, the well-known Kozai mechanism provides an effective migration channel for WD.1856.b. The tidal dissipation that makes this mechanism possible is sensitive to the mass of WD.1856.b, which remains unconstrained by observations. Moreover, the lack of tides in the star allows us to directly connect the current semimajor axis to the pre-migration one, from which we can infer the initial conditions of the system. By further requiring that planets must survive all previous phases of stellar evolution before migrating, we are able to constrain the main-sequence semimajor axis of WD.1856.b to have been similar to 2.5 au, and its mass to be similar or equal to 0.7-3MJ. These mass limits put WD.1856.b firmly within the planet category. Furthermore, our inferred values imply that WD.1856.b was born a typical gas giant. We further estimate the occurrence rate of Kozai-migrated planets around WDs to be O(10(-3) - 10(-4)), suggesting that WD.1856.b is the only one in the TESS sample, but implying. (102) future detections by the LSST survey. In a sense, WD.1856.b was an ordinary Jovian planet that underwent an extraordinary dynamical history.
    ISSN
    2041-8205
    EISSN
    2041-8213
    DOI
    10.3847/2041-8213/abc564
    Version
    Final published version
    Sponsors
    National Science Foundation
    ae974a485f413a2113503eed53cd6c53
    10.3847/2041-8213/abc564
    Scopus Count
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    UA Faculty Publications

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